2005 VX3

2005 VX3 is trans-Neptunian object and retrograde damocloid on a highly eccentric, cometary-like orbit. It was first observed on 1 November 2005, by astronomers with the Mount Lemmon Survey at the Mount Lemmon Observatory in Arizona, United States. The unusual object measures approximately 7 kilometers (4 miles) in diameter.[4] It has the 3rd largest known heliocentric semi-major axis and aphelion.[6] Additionally its perihelion lies within the orbit of Jupiter, which means it also has the largest orbital eccentricity of any known minor planet.

2005 VX3
Discovery [1][2]
Discovered byMount Lemmon Srvy.
Discovery siteMount Lemmon Obs.
(first observed only)
Discovery date1 November 2005
Designations
2005 VX3
TNO [3] · damocloid [4]
unusual [5] · distant [1]
Orbital characteristics [3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc81 days
Aphelion1825.61 AU
Perihelion4.1058 AU
914.86 AU
Eccentricity0.9955
27,672 yr
0.1730°
0° 0m 0s / day
Inclination112.22°
255.35°
196.37°
Jupiter MOID0.8884 AU
TJupiter−0.9430
Physical characteristics
Mean diameter
7 km (est.)[4]
0.09 (assumed)[4]
14.1[1][3]

    Description

    2005 VX3 orbits the Sun at a distance of 4.1–1,826 AU once every 27,672 years (semi-major axis of 915 AU). Its orbit has an eccentricity of 0.9955 and an inclination of 112° with respect to the ecliptic. It belongs to the dynamical group of damocloids due to its retrograde orbit and its low Tisserand parameter (TJupiter of −0.9430).[3] It is a Jupiter-, Saturn-, Uranus-, and Neptune-crosser. The body's observation arc begins with its first observation by the Mount Lemmon Survey on 1 November 2005.[1]

    Orbital evolution — Barycentric elements
    Year[7]
    (epoch)    		AphelionSemimajor-axisRef
    19502710 AUn.a.[lower-alpha 1]
    20121914 AUn.a.[lower-alpha 2]
    20152563 AUn.a.[lower-alpha 3]
    20163235 AUn.a.[lower-alpha 4]
    20502049 AU1026 AU[lower-alpha 1]

    2005 VX3 has a barycentric semi-major axis of ~1026 AU.[7][lower-alpha 1] 2014 FE72 and 2012 DR30 have a larger barycentric semi-major axis. The epoch of January 2016 was when 2005 VX3 had its largest heliocentric semi-major axis.

    The object has a short observation arc of 81 days and does not have a well constrained orbit.[3] It has not been observed since January 2006, when it came to perihelion, 4.1 AU from the Sun.[3] It may be a dormant comet that has not been seen outgassing. In the past it may have made closer approaches to the Sun that could have removed most near-surface volatiles. The current orbit crosses the ecliptic just inside Jupiter's orbit and has a Jupiter-MOID of 0.8 AU.[3]

    In 2017, it had an apparent magnitude of ~28 and was 24 AU from the Sun. It comes to opposition in mid-June. It would require one of the largest telescopes in the world for any more follow-up observations.

    Comparison
    Sedna compared to some other very distant orbiting bodies including 2015 DB216 (orbit wrong), 2000 OO67, 2004 VN112, 2005 VX3, 2006 SQ372, 2007 TG422, 2007 DA61, 2009 MS9, 2010 GB174, 2010 NV1, 2010 BK118, 2012 DR30, 2012 VP113, 2013 BL76, 2013 AZ60, 2013 RF98, 2015 ER61

    See also

    Notes
    1. Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the semi-major axis and orbital period. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates.[8] Using JPL Horizons, the barycentric semi-major axis is approximately 1026 AU.[7]

    References
    1. "2005 VX3". Minor Planet Center. Retrieved 20 November 2018.
    2. "MPEC 2005-V58 : 2005 VX3". IAU Minor Planet Center. 8 November 2005. Retrieved 20 November 2018. (K05V03X)
    3. "JPL Small-Body Database Browser: (2005 VX3)" (2006-01-21 last obs.). Jet Propulsion Laboratory. Retrieved 20 November 2018.
    4. Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 19 November 2018.
    5. "List Of Other Unusual Objects". Minor Planet Center. 14 November 2018. Retrieved 19 November 2018.
    6. "JPL Small-Body Database Search Engine: Asteroids and a > 100 (AU)". JPL Solar System Dynamics. Retrieved 6 March 2014. (Epoch defined at will change every 6 months or so)
    7. Horizons output. "Barycentric Osculating Orbital Elements for 2005 VX3". Retrieved 6 March 2014. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
    8. Kaib, Nathan A.; Becker, Andrew C.; Jones, R. Lynne; Puckett, Andrew W.; Bizyaev, Dmitry; Dilday, Benjamin; et al. (April 2009). "2006 SQ372: A Likely Long-Period Comet from the Inner Oort Cloud". The Astrophysical Journal. 695 (1): 268–275. arXiv:0901.1690. Bibcode:2009ApJ...695..268K. doi:10.1088/0004-637X/695/1/268.

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